含脂肪原发性肝癌的影像诊断及鉴别诊断

目的：探讨CT与MRI对含脂肪原发性肝癌的诊断及鉴别诊断价值。方法：回顾性分析我院病理证实的22例含脂肪原发性肝癌的CT、MRI表现。结果：22例含脂肪肝癌中,巨块型16例,结节型4例,弥漫型2例。肿瘤单发17例,多发5例;5例多发肿瘤内均只有1个含脂肪病灶,共有含脂肪肿瘤22个。18例肿瘤以实质成分为主,肿瘤内脂肪呈散在、小簇状分布;4例肿瘤以脂肪成分为主,瘤内脂肪呈球状表现,实质成分较少。CT显示肿瘤内斑片状、球状脂肪密度影,MRI脂肪抑制序列及化学位移梯度回波序列正反相位均明确显示脂肪的存在。22例动态增强扫描均较好地显示“快进快出”的影像强化特征,其中15例显示肿瘤假性包膜。结论：CT、MRI能较好显示原发性肝癌的影像特征及肿瘤内所含的脂肪组织,对诊断与鉴别诊断具有重要价值。     

弥散加权成像评价直肠癌淋巴结转移的价值

目的：探讨MR弥散加权成像诊断直肠癌淋巴结转移的价值。方法：62例经病理证实直肠癌患者行MRI常规序列扫描及DWI,测量淋巴结ADC值,根据病理结果将MRI检出的淋巴结分为转移性和良性淋巴结两组,将盆腔淋巴结MRI诊断结果与手术病理结果相对照,比较两组淋巴结的ADC值差异是否有统计学意义。结果：共测量225个淋巴结ADC值,b值为800s／mm2,转移性淋巴结组平均ADC值为（0．76±0．15）×10^-3mm2／s,良性淋巴结组平均ADC值为（1．16±0．14）×10^-3mm2／s,两组平均ADC值差异有统计学意义（P〈0．05）。ADC值以1．0×10×10^-3mm2／s为阈值,判断转移性淋巴结与良性淋巴结时,灵敏度、特异度及准确度分别为：94．53％、91．62％和93．45％。结论：弥散加权成像诊断直肠癌淋巴结转移具有较大临床价值。     

多模态影像技术在临床中的应用进展

自人类进入20世纪后,知识结构呈现信息爆炸征象,各项技术迅速发展。PET、PET/CT、PET/MRI、SPECT、SPECT/CT等仪器、技术得以广泛应用,并在疾病诊治等方面取得重大进展。因疾病发生机制较为复杂,各种模态信息量相对单一及片面,存在其自身局限性,使得即使拥有如此多模态的影像技术,仍无法完全实现对复杂疾病的精确评估。故此不同模态图像的信息融合使得信息互补及交叉验证成为可能。该文主要介绍多模态影像技术的发展及应用进展。     

高能双能X射线DR成像及物质识别技术综述

本文关注的是高能双能X射线透视成像以及成像中物体的识别和检测,按照从单能到低能双能再到高能双能的发展脉络介绍了双能X射线DR成像技术背景,详细阐述了高能双能X射线DR成像物质识别原理方法、技术特点和针对性改进,着重讨论了该方法能够用于物质识别的本质,并介绍了该领域面临的挑战和最新进展。     

一种基于平面波静态编码的最小二乘逆时偏移方法

平面波偏移是一种面炮偏移方法,相对于常规逐炮偏移,其具有较高的计算效率.然而常规平面波偏移方法成像精度低,且成像时会产生串扰噪音.为此,本文在实现常规平面波偏移算法基础上,引入反演思想实现了基于静态平面波编码的最小二乘偏移理论方法及处理流程,在优化算法基础上对平层模型和复杂砂砾断块模型进行了成像测试并与其他成像策略进行对比.研究结果表明:基于时移编码的平面波最小二乘偏移能有效抑制低频成像噪音和串扰噪音,补偿中深部成像能量,是一种较为有效的保幅成像策略.     

复杂地表条件下叠前菲涅尔束偏移方法

高斯束偏移虽然克服了Kirchhoff偏移不能处理多波至和单程波动方程偏移不能对陡倾构造准确成像的问题,但在复杂地表条件下其偏移精度取决于所选择的初始束宽度,即当初始宽度较小时,近地表成像精度较高,但此时中深层成像质量较差;反之当初始宽度较大时,中深层成像质量提高,但近地表成像精度降低.针对高斯束偏移中深层和浅层成像精度的矛盾,本文发展了一种适用于陆地复杂地表条件的叠前菲涅尔束偏移方法.基于惠更斯-菲涅尔原理,本文首先给出了菲涅尔束的概念及其表征的格林函数,并采用有效邻域波场近似理论和反褶积成像条件,导出了复杂地表条件下叠前保幅深度偏移公式.最后,针对常规旁轴射线追踪中的数值噪音,给出了一种压制策略.同高斯束偏移相比,本文方法不仅解决了中深层和浅层成像精度的矛盾,而且提高了复杂地表条件下平面波的分解精度,使得偏移结果更加准确可靠.典型的模型算例验证了本文方法的有效性和稳健性.     

Diffraction imaging by uniform asymptotic theory and double exponential fitting

Seismic diffracted waves carry valuable information for identifying geological discontinuities. Unfortunately, the diffraction energy is generally too weak, and standard seismic processing is biased to imaging reflection. In this paper, we present a dynamic diffraction imaging method with the aim of enhancing diffraction and increasing the signal‐to‐noise ratio. The correlation between diffraction amplitudes and their traveltimes generally exists in two forms, with one form based on the Kirchhoff integral formulation, and the other on the uniform asymptotic theory. However, the former will encounter singularities at geometrical shadow boundaries, and the latter requires the computation of a Fresnel integral. Therefore, neither of these methods is appropriate for practical applications. Noting the special form of the Fresnel integral, we propose a least‐squares fitting method based on double exponential functions to study the amplitude function of diffracted waves. The simple form of the fitting function has no singularities and can accelerate the calculation of diffraction amplitude weakening coefficients. By considering both the fitting weakening function and the polarity reversal property of the diffracted waves, we modify the conventional Kirchhoff imaging conditions and formulate a diffraction imaging formula. The mechanism of the proposed diffraction imaging procedure is based on the edge diffractor, instead of the idealized point diffractor. The polarity reversal property can eliminate the background of strong reflection and enhance the diffraction by same‐phase summation. Moreover,the fitting weakening function of diffraction amplitudes behaves like an inherent window to optimize the diffraction imaging aperture by its decaying trend. Synthetic and field data examples reveal that the proposed diffraction imaging method can meet the requirement of high‐resolution imaging, with the edge diffraction fully reinforced and the strong reflection mostly eliminated.     

Fault imaging in sparsely sampled 3D seismic data using common‐reflection‐surface processing and attribute analysis – a study in the Upper Rhine Graben

Cost reduction in seismic reconnaissance is an issue in geothermal exploration and can principally be achieved by sparse acquisition. To address the adherent decrease in signal/noise ratio, the common‐reflection‐surface method has been proposed. We reduced the data density of an existing 3D dataset and evaluated the results of common‐reflection‐surface processing using seismic attributes. The application of the common‐reflection‐surface method leads in all cases to an improvement of the signal/noise ratio. The most distinct improvement can be seen in the low fold regions. The improvement depends strongly on the midpoint aperture, and there is a tradeoff between reflector continuity and horizontal resolution. If small scale targets are to be imaged, a small aperture size is necessary, which may be far below the Fresnel zone for a specific reflector. The substantial reduction of the data density leads in our case to an irrecoverable information loss.     

The chromospherically active binary star EI Eridani: II. Long‐term Doppler imaging

Data from 11 years of continuous spectroscopic observations of the active RS CVn‐type binary star EI Eridani – gained at NSO/McMath‐Pierce, KPNO/Coudé Feed and during the MUSICOS 98 campaign – were used to obtain 34 Doppler maps in three spectroscopic lines for 32 epochs, 28 of which are independent of each other. Various parameters are extracted from our Doppler maps: average temperature, fractional spottedness, and longitudinal and latitudinal spot‐occurrence functions. We find that none of these parameters show a distinct variation nor a correlation with the proposed activity cycle as seen from photometric long‐term observations. This suggests that the photometric brightness cycle may not necessarily be due to just a cool spot cycle. The general morphology of the spot pattern remains persistent over the whole period of 11 years. A large cap‐like polar spot was recovered from all our images. A high degree of variable activity was noticed near latitudes of ≈60–70° where the appendages of the polar spot emerged and dissolved (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Physical properties of morphological units on Comet 9P/Tempel 1 derived from near-IR Deep Impact spectra

In this paper we analyze near-infrared thermal emission spectra of the spatially resolved nucleus of Comet 9P/Tempel 1 obtained by the NASA spacecraft Deep Impact. Maps of spectral reddening, the product X^′ between the beaming function and directional emissivity, as well as surface temperature are constructed. Thermophysical modeling is used to estimate the degree of small scale surface roughness and thermal inertia by detailed reproduction of the empirical temperature map. Mie and Hapke theories are used in combination with numerically calculated beaming functions to analyze the X^′ map and place constraints on composition and grain size of the surface material. We show that it is absolutely mandatory to include small scale surface roughness in thermophysical modeling of this object, since the resulting self heating is vital for reproducing the measured temperatures. A small scale self heating parameter in the range 0.6?ξ?0.75 is common, but smoother areas where 0.2?ξ?0.3 are also found. Contrary to models neglecting small scale surface roughness, we find that the thermal inertia of Comet 9P/Tempel 1 generally is high (1000-3000 J m⁻² K⁻¹ s^−1/2), although it may be substantially lower (40-380 J m⁻² K⁻¹ s^−1/2) in specific areas. We obtain a disk-averaged reddening of 3.5% kÅ⁻¹, with statistically significant local variations around that value on a ±1.0% kÅ−1 level. Vast regions appear covered by small (∼0.1 μm) highly absorbing grains such as carbon or iron-rich silicates. Other regions appear dominated by somewhat larger (∼0.5 μm) and/or less absorbing grains such as troilite or magnesium-rich silicates. Surface variations in reddening, roughness, thermal inertia, composition and/or grain size are moderately to strongly correlated to the locations of morphological units on the surface. The existence of morphological units with differing physical properties may be primordial, hence reflecting a diversity in the building block cometesimals, or resulting from evolutionary processes.